All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f1.ps}\end{figure}$ Figure 1: Background spectra for MOS1. Solid histogram: background spectrum for H between 19-28; squares, triangles and stars: difference of background spectra for H between 29-38, 39-48 and 49-58, respectively, with the 19-28 spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f2.ps}\end{figure}$ Figure 2: Ratio of psf-convolved cluster profile $\phi (r)$ over true cluster profile $\mu (r)$ for MOS1 and a photon energy of 1.5 keV. For $\mu (r)$ we have taken a $\beta$ profile with $\beta =2/3$ and core radii as indicated.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f3.ps}\end{figure}$ Figure 3: Differential emission measure distribution for A 262 in the innermost four shells. Line width decreases with radius; symbols: triangles: 0-0.5 $^\prime$ ; squares: 0.5-1 $^\prime$ ; stars: 1-2 $^\prime$ ; circles: 2-3 $^\prime$ . The dashed line approximates the slope of the isobaric cooling flow model.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f4.ps}\end{figure}$ Figure 4: Differential emission measure distribution for the isobaric cooling flow model, for 0.5 times solar abundances.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f5.ps}\end{figure}$ Figure 5: Spectrum of A 2052 in the inner three shells (with cooling gas). The spectra of all three EPIC camera's have been added. The spectra of the 0.5-1.0 $^\prime$ and 1-2 $^\prime$ shells have been multiplied by factors of 5 and 25, respectively. The spectra are shown as energy times counts/s/keV. Thin solid histograms: fits with a single temperature model; thick solid histograms: fits with the wdem model described in the text.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f6.ps}\end{figure}$ Figure 6: Steepness of the differential emission measure distribution versus cooling time for four clusters as indicated on the plot.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f7.ps}\end{figure}$ Figure 7: Steepness of the differential emission measure distribution versus maximum temperature. The diamonds represent the data points with error bars. The dashed line indicates the weighted average value of $1/\alpha$ , the solid line the best fit power law scaling as described in the text.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f8.ps}\end{figure}$ Figure 8: Scaled temperature profile versus cooling time. Temperatures have been normalised to the temperature $T_{\rm h}$ of the hot gas outside the cooling region. Solid lines, triangles: clusters cooler than 3 keV; dashed lines, squares: clusters with temperatures from 3-4 keV; dash-dotted lines, stars: clusters with temperatures from 4-6 keV; dotted lines, circles: clusters with temperatures above 6 keV. The non-cooling clusters Coma, A754 and A 3266 have been omitted from the plot.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f9.ps}\end{figure}$ Figure 9: Scaled temperature profile versus scaled radius. Temperatures have been normalised as indicated using the temperature $T_{\rm h}$ of the hot gas outside the cooling region as well as the central temperature $T_{\rm c}$ . Triangles: clusters cooler than 3 keV; squares: clusters with temperatures from 3-4 keV; stars: clusters with temperatures from 4-6 keV; circles: clusters with temperatures above 6 keV. The non-cooling clusters Coma, A754 and A 3266 have been omitted from the plot. The solid line is the scaling curve Eq. (10) with $\mu =2$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f10.ps}\end{figure}$ Figure 10: Pressure versus temperature for 16 clusters. Only results for shells where the cooling time is less than 15 Gyr are shown. The center of the cluster is the leftmost data point for each cluster. Pressure and temperature are derived from the isothermal model fits (Table 5).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f11.ps}\end{figure}$ Figure 11: Correlation between the 0.2-10 keV X-ray luminosity within the cooling radius $r_{{\rm cool}}$ as given in Table 11 and $\nu L(\nu )$ at 1.4 GHz for the central radio galaxy. Upper limits are indicated by an arrow.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4230f12.ps}\end{figure}$ Figure 12: The conduction coefficients $\kappa$ required for heat conduction to balance radiation losses as a function of temperature. The solid line is the Spitzer conductivity, the dashed lines are one fifth and one hundredth of the Spitzer conductivity, respectively. Filled diamonds represent the values for the three clusters without cooling flow (Coma, A 3266 and A 754), while open diamonds represent the values for the clusters with a shallow temperature profile (MKW 3s, Sérsic 159-3 and Hydra A). Filled stars represent the remaining clusters. Values for the same cluster are joined by a line and values are given only for bins with cooling times less than $\sim$ 30 Gyr.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f1.ps}\end{figure}$	Figure 1: Background spectra for MOS1. Solid histogram: background spectrum for H between 19-28; squares, triangles and stars: difference of background spectra for H between 29-38, 39-48 and 49-58, respectively, with the 19-28 spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f2.ps}\end{figure}$	Figure 2: Ratio of psf-convolved cluster profile $\phi (r)$ over true cluster profile $\mu (r)$ for MOS1 and a photon energy of 1.5 keV. For $\mu (r)$ we have taken a $\beta$ profile with $\beta =2/3$ and core radii as indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f3.ps}\end{figure}$	Figure 3: Differential emission measure distribution for A 262 in the innermost four shells. Line width decreases with radius; symbols: triangles: 0-0.5 $^\prime$ ; squares: 0.5-1 $^\prime$ ; stars: 1-2 $^\prime$ ; circles: 2-3 $^\prime$ . The dashed line approximates the slope of the isobaric cooling flow model.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f4.ps}\end{figure}$	Figure 4: Differential emission measure distribution for the isobaric cooling flow model, for 0.5 times solar abundances.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f6.ps}\end{figure}$	Figure 6: Steepness of the differential emission measure distribution versus cooling time for four clusters as indicated on the plot.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f7.ps}\end{figure}$	Figure 7: Steepness of the differential emission measure distribution versus maximum temperature. The diamonds represent the data points with error bars. The dashed line indicates the weighted average value of $1/\alpha$ , the solid line the best fit power law scaling as described in the text.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f10.ps}\end{figure}$	Figure 10: Pressure versus temperature for 16 clusters. Only results for shells where the cooling time is less than 15 Gyr are shown. The center of the cluster is the leftmost data point for each cluster. Pressure and temperature are derived from the isothermal model fits (Table 5).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{h4230f11.ps}\end{figure}$	Figure 11: Correlation between the 0.2-10 keV X-ray luminosity within the cooling radius $r_{{\rm cool}}$ as given in Table 11 and $\nu L(\nu )$ at 1.4 GHz for the central radio galaxy. Upper limits are indicated by an arrow.
Open with DEXTER